|Title||Spectroscopy of Dips and Flares in Cir X-1|
|Author||Dr Robert Shirey|
|Description||During dips in Cir X-1, a bright component is obscured, revealing a faint scattered component. Using RXTE, we found a similar Fe Kalpha flux inside and outside dips, suggesting that Fe fluorescence occurs in the scattering medium. We will use EPIC to better constrain physical paramters using this line, and will use RGS to search for other fluorescence lines at lower energy. Our extensive RXTE study also revealed that the flares are associated with branches of a Z-source track. We discovered an unusual line- or edge-like feature near 10 keV on the normal and flaring branches, and our simulations show that the PN could resolve this feature. We have performed extensive simulations of EPIC timing modes in order to confirm that pile-up will not be a problem for PN.|
|Publication||No observations found associated with the current proposal|
|Instrument||EMOS1, EMOS2, EPN, OM, RGS1, RGS2|
|Mission Description||The European Space Agency's (ESA) X-ray Multi-Mirror Mission (XMM-Newton) was launched by an Ariane 504 on December 10th 1999. XMM-Newton is ESA's second cornerstone of the Horizon 2000 Science Programme. It carries 3 high throughput X-ray telescopes with an unprecedented effective area, and an optical monitor, the first flown on a X-ray observatory. The large collecting area and ability to make long uninterrupted exposures provide highly sensitive observations.
Since Earth's atmosphere blocks out all X-rays, only a telescope in space can detect and study celestial X-ray sources. The XMM-Newton mission is helping scientists to solve a number of cosmic mysteries, ranging from the enigmatic black holes to the origins of the Universe itself. Observing time on XMM-Newton is being made available to the scientific community, applying for observational periods on a competitive basis.
|Publisher And Registrant||European Space Agency|
|Credit Guidelines||European Space Agency, 2002-09-17T00:00:00Z, 009452, 17.56_20190403_1200. https://doi.org/10.5270/esa-qjbmel6|